Qatar-1

Last updated
Qatar-1
Observation data
Epoch J2000       Equinox
Constellation Draco
Right ascension 20h 13m 31.6176s
Declination 65° 09′ 43.4909″
Apparent magnitude  (V)12.84
Characteristics
Evolutionary stage main sequence star
Spectral type K3V
B−V color index 1.06
V−R color index 0.19
J−H color index 0.472
J−K color index 0.590
Variable type planetary transit variable
Astrometry
Radial velocity (Rv)-37.835±0.063 km/s
Proper motion (μ)RA: 12.636±0.048  mas/yr
Dec.: 58.170±0.041  mas/yr
Parallax (π)5.3587 ± 0.0231  mas
Distance 609 ± 3  ly
(186.6 ± 0.8  pc)
Details [1] [2]
Mass 0.85±0.03  M☉
Radius 0.823±0.025  R☉
Surface gravity (log g)4.536±0.024  cgs
Temperature 4861±125  K
Metallicity [Fe/H]0.2±0.1  dex
Rotational velocity (v sin i)1.7±0.3 km/s
Age 4.5  Gyr
Other designations
Qatar-1, 2MASS J20133160+6509433, Gaia DR2 2244830490514284928, V592 Dra [3]
Database references
SIMBAD data

Qatar-1 is an orange main sequence star in the constellation of Draco.

Contents

Star characteristics

Qatar-1 has an average to high metallicity of 160% of solar, [1] and is of similar age to Sun. [2] The star has significant starspot activity. [4]

Planetary system

The "Hot Jupiter" class planet Qatar-1b was discovered by the Qatar Exoplanet Survey in 2010. [1] The planetary orbit is likely aligned with the rotational axis of the star, with the misalignment measurement based on the Rossiter-McLaughlin effect equal to −8.4±7.1 degrees. [2] The planet has a large measured temperature difference between dayside (1696±39 K) and nightside (1098±158 K). [5] A spectroscopic study in 2017 does suggest that Qatar-1b has relatively clear skies with a few clouds. [6]

Additional planets or a brown dwarf in the system were suspected in 2013, [7] but were refuted in 2015. [8] [9]

The transit-timing variation search in 2020 has also resulted in no detection of additional planets in the system, [10] [11] although by 2022 additional transit-timing variation data have suggested the planetary system is accelerating under influence of the unseen long-period companion. [12]

The Qatar-1 planetary system [1] [2] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b1.33±0.05  MJ 0.02343±0.00121.4200236±0.0000001 [11] 0.020+0.011
−0.01		84.23±0.06° 1.19±0.09  RJ

Related Research Articles

<span class="mw-page-title-main">TrES-3b</span>

TrES-3b is an extrasolar planet orbiting the star GSC 03089-00929. It has an orbital period of just 31 hours and nearly twice the mass of Jupiter.

<span class="mw-page-title-main">WASP-4b</span> Extrasolar planet in the constellation Phoenix

WASP-4b is an exoplanet, specifically a hot Jupiter, approximately 891 light-years away in the constellation of Phoenix.

WASP-12 is a magnitude 11 yellow dwarf star located approximately 1347 light-years away in the constellation Auriga. WASP-12 has a mass and radius similar to the Sun and is known for being orbited by a planet that is extremely hot and has a retrograde orbit around WASP-12. WASP-12 forms a triple star system with two red dwarf companions. Both of them have spectral types of M3V and are only 38% and 37% as massive as the Sun, respectively.

GSC 03089-00929 is a magnitude 12 star located approximately 757 light-years away in the constellation of Hercules. This star is a G type main sequence star that is similar to but slightly cooler than the Sun. This star is identified in SIMBAD as a variable star per the 1SWASP survey.

HAT-P-12 is a magnitude 13 low-metallicity K dwarf star approximately 463 light years away in the constellation Canes Venatici, which hosts one known exoplanet.

Qatar-2 is a K-type main-sequence star about 595 light-years away in the constellation of Virgo. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.

BD-07 436, also known as WASP-77 since 2012, is a binary star system about 344 light-years away. The star's components appears to have a different age, with the secondary older than 9 billion years, while the primary's age is 5 billion years. The BD-07 436 system's concentration of heavy elements is similar to the Sun. Its stars display moderate chromospheric activity, including x-ray flares.

WASP-64 is a star about 1200 light-years away. It is a G7 class main-sequence star, orbited by a planet WASP-64b. It is younger than the Sun at 3.6±1.6 billion years, and it has a metal abundance similar to the Sun. The star is rotating rapidly, being spun up by the giant planet in a close orbit.

WASP-52 is a K-type main-sequence star about 570 light-years away. It is older than the Sun at 10.7+1.9
−4.5 billion years, but it has a similar fraction of heavy elements. The star has prominent starspot activity, with 3% to 14% of the stellar surface covered by areas 575±150 K cooler than the rest of the photosphere.

Kepler-410 is a binary star system. Its primary star, also known as Kepler-410A, is a F-type subgiant star, orbited by the orange dwarf star Kepler-410B on a wide orbit. The companion star was discovered in 2012.

References

  1. 1 2 3 4 Alsubai, K. A.; Parley, N. R.; Bramich, D. M.; West, R. G.; Sorensen, P. M.; Collier Cameron, A.; Latham, D. W.; Horne, K.; Anderson, D. R.; Bakos, G. Á.; Brown, D. J. A.; Buchhave, L. A.; Esquerdo, G. A.; Everett, M. E.; Fűrész, G.; Hartman, J. D.; Hellier, C.; Miller, G. M.; Pollacco, D.; Quinn, S. N.; Smith, J. C.; Stefanik, R. P.; Szentgyorgyi, A. (2011). "Qatar-1b: A hot Jupiter orbiting a metal-rich K dwarf star". Monthly Notices of the Royal Astronomical Society. 417 (1): 709–716. arXiv: 1012.3027 . Bibcode:2011MNRAS.417..709A. doi: 10.1111/j.1365-2966.2011.19316.x . S2CID   55675165.
  2. 1 2 3 4 Covino, E.; Esposito, M.; Barbieri, M.; Mancini, L.; Nascimbeni, V.; Claudi, R.; Desidera, S.; Gratton, R.; Lanza, A. F.; Sozzetti, A.; Biazzo, K.; Affer, L.; Gandolfi, D.; Munari, U.; Pagano, I.; Bonomo, A. S.; Collier Cameron, A.; Hébrard, G.; Maggio, A.; Messina, S.; Micela, G.; Molinari, E.; Pepe, F.; Piotto, G.; Ribas, I.; Santos, N. C.; Southworth, J.; Shkolnik, E.; Triaud, A. H. M. J.; et al. (2013). "The GAPS programme with HARPS-N at TNG". Astronomy & Astrophysics. 554: A28. arXiv: 1304.0005 . doi:10.1051/0004-6361/201321298. S2CID   54793301.
  3. ↑ Qatar 1 -- High proper-motion Star
  4. ↑ Mislis, D.; Mancini, L.; Tregloan-Reed, J.; Ciceri, S.; Southworth, J.; d'Ago, G.; Bruni, I.; Baştürk, Ö.; Alsubai, K. A.; Bachelet, E.; Bramich, D. M.; Henning, Th.; Hinse, T. C.; Iannella, A. L.; Parley, N.; Schroeder, T. (2015). "High-precision multiband time series photometry of exoplanets Qatar-1b and TrES-5b". Monthly Notices of the Royal Astronomical Society. 448 (3): 2617–2623. arXiv: 1503.02246 . Bibcode:2015MNRAS.448.2617M. doi: 10.1093/mnras/stv197 . S2CID   53561305.
  5. ↑ May, Erin; Stevenson, Kevin; Bean, Jacob; Bell, Taylor; Cowan, Nicolas; Dang, Lisa; Desert, Jean-Michel; Fortney, Jonathan; Keating, Dylan; Kempton, Eliza; Komacek, Thaddeus; Lewis, Nikole; Mansfield, Megan; Morley, Caroline; Parmentier, Vivien; Rauscher, Emily; Swain, Mark; Zellem, Robert; Showman, Adam (2022), "A New Analysis of Eight Spitzer Phase Curves and Hot Jupiter Population Trends: Qatar-1b, Qatar-2b, WASP-52b, WASP-34b, and WASP-140b", The Astronomical Journal, 163 (6): 256, arXiv: 2203.15059 , Bibcode:2022AJ....163..256M, doi: 10.3847/1538-3881/ac6261 , S2CID   247778438
  6. ↑ von Essen, C.; Cellone, S.; Mallonn, M.; Albrecht, S.; Miculán, R.; Müller, H. M. (2017). "Testing connections between exo-atmospheres and their host stars". Astronomy & Astrophysics. 603: A20. arXiv: 1703.10647 . doi:10.1051/0004-6361/201730506. S2CID   119452420.
  7. ↑ von Essen, C.; Schröter, S.; Agol, E.; Schmitt, J. H. M. M. (2013). "Qatar-1: Indications for possible transit timing variations". Astronomy & Astrophysics. 555: A92. arXiv: 1309.1457 . Bibcode:2013A&A...555A..92V. doi:10.1051/0004-6361/201321407. S2CID   119174903.
  8. ↑ MacIejewski, G.; Fernández, M.; Aceituno, F. J.; Ohlert, J.; Puchalski, D.; Dimitrov, D.; Seeliger, M.; Kitze, M.; Raetz, St.; Errmann, R.; Gilbert, H.; Pannicke, A.; Schmidt, J.-G.; Neuhäuser, R. (2015). "No variations in transit times for Qatar-1 B". Astronomy & Astrophysics. 577: A109. arXiv: 1503.07191 . Bibcode:2015A&A...577A.109M. doi:10.1051/0004-6361/201526031. S2CID   118638934.
  9. ↑ Collins, Karen A.; Kielkopf, John F.; Stassun, Keivan G. (2015). "TRANSIT TIMING VARIATION MEASUREMENTS OF WASP-12b AND QATAR-1b: NO EVIDENCE OF ADDITIONAL PLANETS". The Astronomical Journal. 153 (2): 78. arXiv: 1512.00464 . doi: 10.3847/1538-3881/153/2/78 . S2CID   55191644.
  10. 1 2 Thakur, Parijat; Mannaday, Vineet Kumar; Sahu, Devendra Kumar; Chand, Swadesh; Jiang, Ing-Guey (2020), "Investigating Extra-solar Planetary System Qatar-1 through Transit Observations", Bulletin de la Société Royale des Sciences de Liège: 132–136, arXiv: 2007.03753 , doi:10.25518/0037-9565.7577, S2CID   54660279
  11. 1 2 Su, Li-Hsin; Jiang, Ing-Guey; Sariya, Devesh P.; Lee, Chiao-Yu; Yeh, Li-Chin; Mannaday, Vineet Kumar; Thakur, Parijat; Sahu, D. K.; Chand, Swadesh; Shlyapnikov, A. A.; Moskvin, V. V.; Ignatov, Vladimir; Mkrtichian, David; Griv, Evgeny (2021), "Are There Transit Timing Variations for the Exoplanet Qatar-1b?", The Astronomical Journal, 161 (3): 108, arXiv: 2012.08184 , Bibcode:2021AJ....161..108S, doi: 10.3847/1538-3881/abd4d8 , S2CID   229181287
  12. ↑ Mannaday, Vineet Kumar; Thakur, Parijat; Southworth, John; Jiang, Ing-Guey; Sahu, D. K.; Mancini, L.; Vaňko, M.; Kundra, Emil; Gajdoš, Pavol; a-Thano, Napaporn; Sariya, Devesh P.; Yeh, Li-Chin; Griv, Evgeny; Mkrtichian, David; Shlyapnikov, Aleksey (2022), "Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data", The Astronomical Journal, 164 (5): 198, arXiv: 2209.04080 , Bibcode:2022AJ....164..198M, doi: 10.3847/1538-3881/ac91c2 , S2CID   252185524


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